Why Is Mars Orange?
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Chemical Variations in Yellowknife Bay Formation Sedimentary Rocks
PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Chemical variations in Yellowknife Bay formation 10.1002/2014JE004681 sedimentary rocks analyzed by ChemCam Special Section: on board the Curiosity rover on Mars Results from the first 360 Sols of the Mars Science Laboratory N. Mangold1, O. Forni2, G. Dromart3, K. Stack4, R. C. Wiens5, O. Gasnault2, D. Y. Sumner6, M. Nachon1, Mission: Bradbury Landing P.-Y. Meslin2, R. B. Anderson7, B. Barraclough4, J. F. Bell III8, G. Berger2, D. L. Blaney9, J. C. Bridges10, through Yellowknife Bay F. Calef9, B. Clark11, S. M. Clegg5, A. Cousin5, L. Edgar8, K. Edgett12, B. Ehlmann4, C. Fabre13, M. Fisk14, J. Grotzinger4, S. Gupta15, K. E. Herkenhoff7, J. Hurowitz16, J. R. Johnson17, L. C. Kah18, N. Lanza19, Key Points: 2 1 20 21 12 16 2 • J. Lasue , S. Le Mouélic , R. Léveillé , E. Lewin , M. Malin , S. McLennan , S. Maurice , Fluvial sandstones analyzed by 22 22 23 19 19 24 25 ChemCam display subtle chemical N. Melikechi , A. Mezzacappa , R. Milliken , H. Newsom , A. Ollila , S. K. Rowland , V. Sautter , variations M. Schmidt26, S. Schröder2,C.d’Uston2, D. Vaniman27, and R. Williams27 • Combined analysis of chemistry and texture highlights the role of 1Laboratoire de Planétologie et Géodynamique de Nantes, CNRS, Université de Nantes, Nantes, France, 2Institut de Recherche diagenesis en Astrophysique et Planétologie, CNRS/Université de Toulouse, UPS-OMP, Toulouse, France, 3Laboratoire de Géologie de • Distinct chemistry in upper layers 4 5 suggests distinct setting and/or Lyon, Université de Lyon, Lyon, France, California Institute of Technology, Pasadena, California, USA, Los Alamos National 6 source Laboratory, Los Alamos, New Mexico, USA, Earth and Planetary Sciences, University of California, Davis, California, USA, 7Astrogeology Science Center, U.S. -
Transit Timing Analysis of the Hot Jupiters WASP-43B and WASP-46B and the Super Earth Gj1214b
Transit timing analysis of the hot Jupiters WASP-43b and WASP-46b and the super Earth GJ1214b Mathias Polfliet Promotors: Michaël Gillon, Maarten Baes 1 Abstract Transit timing analysis is proving to be a promising method to detect new planetary partners in systems which already have known transiting planets, particularly in the orbital resonances of the system. In these resonances we might be able to detect Earth-mass objects well below the current detection and even theoretical (due to stellar variability) thresholds of the radial velocity method. We present four new transits for WASP-46b, four new transits for WASP-43b and eight new transits for GJ1214b observed with the robotic telescope TRAPPIST located at ESO La Silla Observatory, Chile. Modelling the data was done using several Markov Chain Monte Carlo (MCMC) simulations of the new transits with old data and a collection of transit timings for GJ1214b from published papers. For the hot Jupiters this lead to a general increase in accuracy for the physical parameters of the system (for the mass and period we found: 2.034±0.052 MJup and 0.81347460±0.00000048 days and 2.03±0.13 MJup and 1.4303723±0.0000011 days for WASP-43b and WASP-46b respectively). For GJ1214b this was not the case given the limited photometric precision of TRAPPIST. The additional timings however allowed us to constrain the period to 1.580404695±0.000000084 days and the RMS of the TTVs to 16 seconds. We investigated given systems for Transit Timing Variations (TTVs) and variations in the other transit parameters and found no significant (3sv) deviations. -
ROVING ACROSS MARS: SEARCHING for EVIDENCE of FORMER HABITABLE ENVIRONMENTS Michael H
PERSPECTIVE ROVING ACROSS MARS: SEARCHING FOR EVIDENCE OF FORMER HABITABLE ENVIRONMENTS Michael H. Carr* My love affair with Mars started in the late 1960s when I was appointed a member of the Mariner 9 and Viking Orbiter imaging teams. The global surveys of these two missions revealed a geological wonderland in which many of the geological processes that operate here on Earth operate also on Mars, but on a grander scale. I was subsequently involved in almost every Mars mission, both US and non- US, through the early 2000s, and wrote several books on Mars, most recently The Surface of Mars (Carr 2006). I also participated extensively in NASA’s long-range strategic planning for Mars exploration, including assessment of the merits of various techniques, such as penetrators, Mars rovers showing their evolution from 1996 to the present day. FIGURE 1 balloons, airplanes, and rovers. I am, therefore, following the results In the foreground is the tethered rover, Sojourner, launched in 1996. On the left is a model of the rovers Spirit and Opportunity, launched in 2004. from Curiosity with considerable interest. On the right is Curiosity, launched in 2011. IMAGE CREDIT: NASA/JPL-CALTECH The six papers in this issue outline some of the fi ndings of the Mars rover Curiosity, which has spent the last two years on the Martian surface looking for evidence of past habitable conditions. It is not the fi rst rover to explore Mars, but it is by far the most capable (FIG. 1). modest-sized landed vehicles. Advances in guidance enabled landing Included on the vehicle are a number of cameras, an alpha particle at more interesting and promising places, and advances in robotics led X-ray spectrometer (APXS) for contact elemental composition, a spec- to vehicles with more independent capabilities. -
Mars Science Laboratory: Curiosity Rover Curiosity’S Mission: Was Mars Ever Habitable? Acquires Rock, Soil, and Air Samples for Onboard Analysis
National Aeronautics and Space Administration Mars Science Laboratory: Curiosity Rover www.nasa.gov Curiosity’s Mission: Was Mars Ever Habitable? acquires rock, soil, and air samples for onboard analysis. Quick Facts Curiosity is about the size of a small car and about as Part of NASA’s Mars Science Laboratory mission, Launch — Nov. 26, 2011 from Cape Canaveral, tall as a basketball player. Its large size allows the rover Curiosity is the largest and most capable rover ever Florida, on an Atlas V-541 to carry an advanced kit of 10 science instruments. sent to Mars. Curiosity’s mission is to answer the Arrival — Aug. 6, 2012 (UTC) Among Curiosity’s tools are 17 cameras, a laser to question: did Mars ever have the right environmental Prime Mission — One Mars year, or about 687 Earth zap rocks, and a drill to collect rock samples. These all conditions to support small life forms called microbes? days (~98 weeks) help in the hunt for special rocks that formed in water Taking the next steps to understand Mars as a possible and/or have signs of organics. The rover also has Main Objectives place for life, Curiosity builds on an earlier “follow the three communications antennas. • Search for organics and determine if this area of Mars was water” strategy that guided Mars missions in NASA’s ever habitable for microbial life Mars Exploration Program. Besides looking for signs of • Characterize the chemical and mineral composition of Ultra-High-Frequency wet climate conditions and for rocks and minerals that ChemCam Antenna rocks and soil formed in water, Curiosity also seeks signs of carbon- Mastcam MMRTG • Study the role of water and changes in the Martian climate over time based molecules called organics. -
EGU2015-6247, 2015 EGU General Assembly 2015 © Author(S) 2015
Geophysical Research Abstracts Vol. 17, EGU2015-6247, 2015 EGU General Assembly 2015 © Author(s) 2015. CC Attribution 3.0 License. From Kimberley to Pahrump_Hills: toward a working sedimentary model for Curiosity’s exploration of strata from Aeolis Palus to lower Mount Sharp in Gale crater Sanjeev Gupta (1), David Rubin (2), Katie Stack (3), John Grotzinger (4), Rebecca Williams (5), Lauren Edgar (6), Dawn Sumner (7), Melissa Rice (8), Kevin Lewis (9), Michelle Minitti (5), Juergen Schieber (10), Ken Edgett (11), Ashwin Vasawada (3), Marie McBride (11), Mike Malin (11), and the MSL Science Team (1) Imperial College London, London, United Kingdom ([email protected]), (2) UC, Santa Cruz, CA, USA, (3) Jet Propulsion Laboratory, Pasadena, CA, USA, (4) California Institute of Technology, Pasadena, CA, USA, (5) Planetary Science INstitute, Tucson, AZ, USA, (6) USGS, Flagstaff, AZ, USA, (7) UC, Davis, CA, USA, (8) Western Washington University, Bellingham, WA, USA, (9) Johns Hopkins University, Baltimore, Maryland, USA, (10) Indiana University, Bloomington, Indiana, USA, (11) Malin Space Science Systems, San Diego, CA, USA In September 2014, NASA’s Curiosity rover crossed the transition from sedimentary rocks of Aeolis Palus to those interpreted to be basal sedimentary rocks of lower Aeolis Mons (Mount Sharp) at the Pahrump Hills outcrop. This transition records a change from strata dominated by coarse clastic deposits comprising sandstones and conglomerate facies to a succession at Pahrump Hills that is dominantly fine-grained mudstones and siltstones with interstratified sandstone beds. Here we explore the sedimentary characteristics of the deposits, develop depositional models in the light of observed physical characteristics and develop a working stratigraphic model to explain stratal relationships. -
JSC-Rocknest: a Large-Scale Mojave Mars Simulant (MMS) Based Soil Simulant for In-Situ
1 JSC-Rocknest: A large-scale Mojave Mars Simulant (MMS) based soil simulant for in-situ 2 resource utilization water-extraction studies 3 Clark, J.V.a*, Archer, P.D.b, Gruener, J.E.c, Ming, D.W.c, Tu, V.M.b, Niles, P.B.c, Mertzman, 4 S.A.d 5 a GeoControls Systems, Inc – Jacobs JETS Contract at NASA Johnson Space Center, 2101 6 NASA Pkwy, Houston, TX 77058, USA. [email protected], 281-244-7442 7 b Jacobs JETS Contract at NASA Johnson Space Center, 2101 NASA Pkwy, Houston, TX 8 77058, USA. 9 c NASA Johnson Space Center, 2101 NASA Pkwy, Houston, TX 77058, USA. 10 d Department of Earth and Environmental, Franklin & Marshall College, Lancaster, PA 17604, 11 USA. 12 *Corresponding author 13 14 15 16 17 18 19 Keywords: Simulant, Mars, In-situ resource utilization, evolved gas analysis, Rocknest 1 20 Abstract 21 The Johnson Space Center-Rocknest (JSC-RN) simulant was developed in response to a 22 need by NASA's Advanced Exploration Systems (AES) In-Situ Resource Utilization (ISRU) 23 project for a simulant to be used in component and system testing for water extraction from Mars 24 regolith. JSC-RN was designed to be chemically and mineralogically similar to material from the 25 aeolian sand shadow named Rocknest in Gale Crater, particularly the 1-3 wt.% low temperature 26 (<450 ºC) water release as measured by the Sample Analysis at Mars (SAM) instrument on the 27 Curiosity rover. Sodium perchlorate, goethite, pyrite, ferric sulfate, regular and high capacity 28 granular ferric oxide, and forsterite were added to a Mojave Mars Simulant (MMS) base in order 29 to match the mineralogy, evolved gases, and elemental chemistry of Rocknest. -
Abstracts of the 50Th DDA Meeting (Boulder, CO)
Abstracts of the 50th DDA Meeting (Boulder, CO) American Astronomical Society June, 2019 100 — Dynamics on Asteroids break-up event around a Lagrange point. 100.01 — Simulations of a Synthetic Eurybates 100.02 — High-Fidelity Testing of Binary Asteroid Collisional Family Formation with Applications to 1999 KW4 Timothy Holt1; David Nesvorny2; Jonathan Horner1; Alex B. Davis1; Daniel Scheeres1 Rachel King1; Brad Carter1; Leigh Brookshaw1 1 Aerospace Engineering Sciences, University of Colorado Boulder 1 Centre for Astrophysics, University of Southern Queensland (Boulder, Colorado, United States) (Longmont, Colorado, United States) 2 Southwest Research Institute (Boulder, Connecticut, United The commonly accepted formation process for asym- States) metric binary asteroids is the spin up and eventual fission of rubble pile asteroids as proposed by Walsh, Of the six recognized collisional families in the Jo- Richardson and Michel (Walsh et al., Nature 2008) vian Trojan swarms, the Eurybates family is the and Scheeres (Scheeres, Icarus 2007). In this theory largest, with over 200 recognized members. Located a rubble pile asteroid is spun up by YORP until it around the Jovian L4 Lagrange point, librations of reaches a critical spin rate and experiences a mass the members make this family an interesting study shedding event forming a close, low-eccentricity in orbital dynamics. The Jovian Trojans are thought satellite. Further work by Jacobson and Scheeres to have been captured during an early period of in- used a planar, two-ellipsoid model to analyze the stability in the Solar system. The parent body of the evolutionary pathways of such a formation event family, 3548 Eurybates is one of the targets for the from the moment the bodies initially fission (Jacob- LUCY spacecraft, and our work will provide a dy- son and Scheeres, Icarus 2011). -
Self-Organizing Systems in Planetary Physics: Harmonic Resonances Of
Self-Organizing Systems in Planetary Physics : Harmonic Resonances of Planet and Moon Orbits Markus J. Aschwanden1 1) Lockheed Martin, Solar and Astrophysics Laboratory, Org. A021S, Bldg. 252, 3251 Hanover St., Palo Alto, CA 94304, USA; e-mail: [email protected] ABSTRACT The geometric arrangement of planet and moon orbits into a regularly spaced pattern of distances is the result of a self-organizing system. The positive feedback mechanism that operates a self-organizing system is accomplished by harmonic orbit resonances, leading to long-term stable planet and moon orbits in solar or stellar systems. The distance pattern of planets was originally described by the empirical Titius-Bode law, and by a generalized version with a constant geometric progression factor (corresponding to logarithmic spacing). We find that the orbital periods Ti and planet distances Ri from the Sun are not consistent with logarithmic spacing, 2/3 2/3 but rather follow the quantized scaling (Ri+1/Ri) = (Ti+1/Ti) = (Hi+1/Hi) , where the harmonic ratios are given by five dominant resonances, namely (Hi+1 : Hi)=(3:2), (5 : 3), (2 : 1), (5 : 2), (3 : 1). We find that the orbital period ratios tend to follow the quantized harmonic ratios in increasing order. We apply this harmonic orbit resonance model to the planets and moons in our solar system, and to the exo-planets of 55 Cnc and HD 10180 planetary systems. The model allows us a prediction of missing planets in each planetary system, based on the quasi- regular self-organizing pattern of harmonic orbit resonance zones. We predict 7 (and 4) missing exo-planets around the star 55 Cnc (and HD 10180). -
Astro Vol.7 Issue 4
NEWSLETTER Year 7, Issue 04 PSSP - News The First NASA Videoconference Prepared by Elzbieta Gwiazda-Szer On the 15th of January there was a videoconference between the Rota College (Izmir, Turkey), School4Child (Lodz, Poland) and NASA’s Marshall Space Flight Center in Huntsville, Alabama in the U.S.A.. It was a historical day for both schools since it was their first videoconference with a NASA Center. Our school prepared for that during the classes conducted by Ms. Elzbieta Gwiazda-Szer . The classes and videoconference’s theme was "Toys in Space". In class, students got familiar with Newton's three principles of dynamics, they learned about gravity and microgravity. In groups, students sought answers to questions concerning the behavior of their toys in space. Their considerations related to a football , a jump rope , a kendama and a paper boomerang . Some students have modified their toys in order to improve the fun efficiency in microgravity. Our students also had the opportunity to meet with their ePals, with whom they are in touch via emails. This is the third year we have been partners of the program PSSP - Partner School Science Program. The videoconferencing has been received with great enthusiasm by both our students and students from Turkey. Pages 1 Technology Lunar Time Lapse Panorama including Yutu Rover Image Credit: CNSA, Chinanews, Kenneth Kremer & Marco Di Lorenzo Where has the Yutu rover been on the Moon? Arriving in 2013 mid-December, the Chinese Yutu robotic rover has spent some of the past month and a half exploring Mare Imbrium on Earth's Moon. -
Filipiak Solar System Book
Our Solar System Mrs. Filipiak’s Class Our Solar System Mrs. Filipiak’s Class Sun ...............................................................................................7 Michael ........................................................................................7 Mercury ........................................................................................1 Denzel ..........................................................................................1 Mercury ........................................................................................3 Austin ...........................................................................................3 Mercury ........................................................................................5 Madison B ....................................................................................5 Venus ............................................................................................7 Shyla .............................................................................................7 Venus ............................................................................................9 Kenny ...........................................................................................9 Earth ..........................................................................................11 Kaleb ..........................................................................................11 Earth ..........................................................................................13 -
A Miniaturized Chemin Xrd/Xrf for Future Mars Exploration
Ninth International Conference on Mars 2019 (LPI Contrib. No. 2089) 6230.pdf A MINIATURIZED CHEMIN XRD/XRF FOR FUTURE MARS EXPLORATION. B. Lafuente1, P. Sarrazin1, T. F. Bristow2, D. F. Blake2, M. Gailhanou3, J. Chen4, K. Thompson1, R. Walroth2, K. Zacny5, R. T. Downs6, and A. Yen7, 1SETI Institute, Mountain View, CA ([email protected]), 2Exobiology, NASA ARC, Moffett Field, CA, 3CNRS, IM2NP UMR, Marseille, France, 4Baja Technology, Tempe, AZ, 5Honeybee Robotics Spacecraft Mecha- nisms Corp., Pasadena, CA, 6Geosciences, Univ. Arizona, Tucson AZ, 7JPL, Pasadena, CA. Introduction: X-ray Diffraction (XRD) and X-ray ergy-selective detection of XRD photons in Mars’ ra- Fluorescence (XRF) analyses provide the most diag- diative environment. The CheMinX XRD geometry is nostic and complete characterization of rocks and soil based on an architecture demonstrated by hundreds of by any spacecraft-capable technique, improved upon commercial XRD instruments (Terra, commercial spin- only by sample return and analysis in terrestrial labora- off of CheMin, Fig. 1). This design resulted from a tories. In a complex sample such as a basalt, XRD can ray-tracing study of XRD geometries based on high as- definitively identify and quantify all minerals, establish pect-ratio detectors. It was found that reduced surface their individual elemental compositions and quantify area detectors can be used with no loss in throughput, the amount of the amorphous component. When cou- angular resolution or angular range, the loss in detector pled with XRF, the composition of the amorphous coverage being fully compensated for by an optimized component can be determined as well. collimator design. The MSL CheMin instrument, the first XRD instru- In its basic implementation CheMinX will provide ment flown in space, established the quantitative min- a resolution of 0.3° 2θ FWHM, slightly improved over eralogy of the Mars soil [1], characterized the first hab- CheMin’s 0.35°. -
Determining Mineralogy on Mars with the Chemin X-Ray Diffractometer the Chemin Team Logo Illustrating the Diffraction of Minerals on Mars
Determining Mineralogy on Mars with the CheMin X-Ray Diffractometer The CheMin team logo illustrating the diffraction of minerals on Mars. Robert T. Downs1 and the MSL Science Team 1811-5209/15/0011-0045$2.50 DOI: 10.2113/gselements.11.1.45 he rover Curiosity is conducting X-ray diffraction experiments on the The mineralogy of the Martian surface of Mars using the CheMin instrument. The analyses enable surface is dominated by the phases found in basalt and its ubiquitous Tidentifi cation of the major and minor minerals, providing insight into weathering products. To date, the the conditions under which the samples were formed or altered and, in turn, major basaltic minerals identi- into past habitable environments on Mars. The CheMin instrument was devel- fied by CheMin include Mg– Fe-olivines, Mg–Fe–Ca-pyroxenes, oped over a twenty-year period, mainly through the efforts of scientists and and Na–Ca–K-feldspars, while engineers from NASA and DOE. Results from the fi rst four experiments, at the minor primary minerals include Rocknest, John Klein, Cumberland, and Windjana sites, have been received magnetite and ilmenite. CheMin and interpreted. The observed mineral assemblages are consistent with an also identifi ed secondary minerals formed during alteration of the environment hospitable to Earth-like life, if it existed on Mars. basalts, such as calcium sulfates KEYWORDS: X-ray diffraction, Mars, Gale Crater, habitable environment, CheMin, (anhydrite and bassanite), iron Curiosity rover oxides (hematite and akaganeite), pyrrhotite, clays, and quartz. These secondary minerals form and INTRODUCTION persist only in limited ranges of temperature, pressure, and The Mars rover Curiosity landed in Gale Crater on August ambient chemical conditions (i.e.